The nuclear stellar disc ( NSD ) is a flattened stellar structure that dominates the gravitational potential of the Milky Way at Galactocentric radii 30 \lesssim R \lesssim 300 { pc } . In this paper , we construct axisymmetric Jeans dynamical models of the NSD based on previous photometric studies and we fit them to line-of-sight kinematic data of APOGEE and SiO masers stars . We find that ( i ) the NSD mass is lower but consistent with the mass independently determined from photometry by Launhardt et al . ( 2002 ) . Our fiducial model has a mass contained within spherical radius r = 100 { pc } of M ( r < 100 { pc } ) = 3.9 \pm 1 \times 10 ^ { 8 } M _ { \odot } and a total mass of M _ { NSD } = 6.9 \pm 2 \times 10 ^ { 8 } M _ { \odot } . ( ii ) The NSD might be the first example of a vertically biased disc , i.e . with ratio between the vertical and radial velocity dispersion \sigma _ { z } / \sigma _ { R } > 1 . Observations and theoretical models of the star-forming molecular gas in the central molecular zone suggest that large vertical oscillations may be already imprinted at stellar birth . However , the finding \sigma _ { z } / \sigma _ { R } > 1 depends on a drop in the velocity dispersion in the innermost few tens of parsecs , on our assumption that the velocity ellipsoid is aligned on cylindrical coordinates , and that the available ( extinction corrected ) stellar samples broadly trace the underlying light and mass distributions , all of which need to be established by future observations and/or modelling . ( iii ) We provide the most accurate rotation curve to date for the innermost 500 { pc } of our Galaxy .