We present two-dimensional stellar and gaseous kinematics of the inner 0.8 \times 1.1 kpc ^ { 2 } of the LINER/Seyfert 1 galaxy NGC 7213 , from optical spectra obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of \approx 60 pc . The stellar kinematics shows an average velocity dispersion of 177 km s ^ { -1 } , circular rotation with a projected velocity amplitude of 50 km s ^ { -1 } and a kinematic major axis at a position angle of \approx -4 ^ { \circ } ( west of north ) . From the average velocity dispersion we estimate a black hole mass of M _ { BH } = 8 _ { -6 } ^ { +16 } \times 10 ^ { 7 } M _ { \odot } . The gas kinematics is dominated by non-circular motions , mainly along two spiral arms extending from the nucleus out to \approx 4″ ( 280 pc ) to the NW and SE , that are cospatial with a nuclear dusty spiral seen in a structure map of the nuclear region of the galaxy . The projected gas velocities along the spiral arms show blueshifts in the far side and redshifts in the near side , with values of up to 200 km s ^ { -1 } . This kinematics can be interpreted as gas inflows towards the nucleus along the spiral arms if the gas is in the plane of the galaxy . We estimate the mass inflow rate using two different methods . The first is based of the observed velocities and geometry of the flow , and gives a mass inflow rate in the ionised gas of \approx 7 \times 10 ^ { -2 } M _ { \odot } yr ^ { -1 } . In the second method , we calculate the net ionised gas mass flow rate through concentric circles of decreasing radii around the nucleus resulting in mass inflow rates ranging from \approx 0.4 M _ { \odot } yr ^ { -1 } at 300 pc down to \approx 0.2 M _ { \odot } yr ^ { -1 } at 100 pc from the nucleus . These rates are larger than necessary to power the active nucleus .