Context : Aims : We investigate the fueling and the feedback of star formation and nuclear activity in NGC 1068 , a nearby ( D = 14 Mpc ) Seyfert 2 barred galaxy , by analyzing the distribution and kinematics of the molecular gas in the disk . We aim to understand if and how gas accretion can self-regulate . Methods : We have used the Atacama Large Millimeter Array ( ALMA ) to map the emission of a set of dense molecular gas ( n ( H _ { 2 } ) \simeq 10 ^ { 5 - 6 } cm ^ { -3 } ) tracers ( CO ( 3–2 ) , CO ( 6–5 ) , HCN ( 4–3 ) , HCO ^ { + } ( 4–3 ) , and CS ( 7–6 ) ) and their underlying continuum emission in the central r \sim 2 kpc of NGC 1068 with spatial resolutions \sim 0.3 \arcsec - 0.5 \arcsec ( \sim 20 - 35 pc for the assumed distance of D = 14 Mpc ) . Results : The sensitivity and spatial resolution of ALMA give an unprecedented detailed view of the distribution and kinematics of the dense molecular gas ( n ( H _ { 2 } ) \geq 10 ^ { 5 - 6 } cm ^ { -3 } ) in NGC 1068 . Molecular line and dust continuum emissions are detected from a r \sim 200 pc off-centered circumnuclear disk ( CND ) , from the 2.6 kpc-diameter bar region , and from the r \sim 1.3 kpc starburst ( SB ) ring . Most of the emission in HCO ^ { + } , HCN , and CS stems from the CND . Molecular line ratios show dramatic order-of-magnitude changes inside the CND that are correlated with the UV/X-ray illumination by the AGN , betraying ongoing feedback . We used the dust continuum fluxes measured by ALMA together with NIR/MIR data to constrain the properties of the putative torus using CLUMPY models and found a torus radius of 20 ^ { +6 } _ { -10 } pc . The Fourier decomposition of the gas velocity field indicates that rotation is perturbed by an inward radial flow in the SB ring and the bar region . However , the gas kinematics from r \sim 50 pc out to r \sim 400 pc reveal a massive ( M _ { mol } \sim 2.7 ^ { +0.9 } _ { -1.2 } \times 10 ^ { 7 } M _ { \sun } ) outflow in all molecular tracers . The tight correlation between the ionized gas outflow , the radio jet , and the occurrence of outward motions in the disk suggests that the outflow is AGN driven . Conclusions : The molecular outflow is likely launched when the ionization cone of the narrow line region sweeps the nuclear disk . The outflow rate estimated in the CND , \mathrm { d } M / \mathrm { d } t \sim 63 ^ { +21 } _ { -37 } ~ { } M _ { \odot } yr ^ { -1 } , is an order of magnitude higher than the star formation rate at these radii , confirming that the outflow is AGN driven . The power of the AGN is able to account for the estimated momentum and kinetic luminosity of the outflow . The CND mass load rate of the CND outflow implies a very short gas depletion timescale of \leq 1 Myr . The CND gas reservoir is likely replenished on longer timescales by efficient gas inflow from the outer disk .