  The nuclear stellar disc (NSD) is a flattened stellar structure that
dominates the gravitational potential of the Milky Way at Galactocentric radii
$30 \lesssim R \lesssim 300{\, \rm pc}$. 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 maser
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 $r=100{\, \rm pc}$
of $M(r<100{\, \rm pc}) = 3.9 \pm 1 \times 10^8 {\, \rm M_\odot}$ and a total
mass of $M_{\rm NSD} = 6.9 \pm 2 \times 10^8 {\, \rm M_\odot}$. (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 NSD is axisymmetric, 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 $500 {\, \rm pc}$ of our Galaxy.
