  We use data from the Gaia DR3 dataset to estimate the mass of the Milky Way
(MW) by analyzing the rotation curve in the range of distances 5 kpc to 28 kpc.
We consider three mass models: the first model adds a spherical dark matter
(DM) halo, following the Navarro-Frenk-White (NFW) profile, to the known
stellar components. The second model assumes that DM is confined to the
Galactic disk, following the idea that the observed density of gas in the
Galaxy is related to the presence of more massive DM disk (DMD), similar to the
observed correlation between DM and gas in other galaxies. The third model only
uses the known stellar mass components and is based on the Modified Newton
Dynamics (MOND) theory. Our results indicate that the DMD model is comparable
in accuracy to the NFW and MOND models and fits the data better at large radii
where the rotation curve declines but has the largest errors. For the NFW model
we obtain a virial mass $M_{vir}= (6.5 \pm 0.3) \times 10^{11} \; M_\odot$ with
concentration parameter $c=14.5$, that is lower than what is typically
reported. In the DMD case we find that the MW mass is $M_d = (1.6 \pm 0.5)
\times 10^{11} \; M_\odot$ with a disk's characteristic radius of $R_d=17$ kpc.
