  With the release of Gaia DR3, we extend the comparison between dynamical
models for the Milky Way rotation curve initiated in the previous work.
Utilising astrometric and spectro-photometric data for 719143 young disc stars
within $|z|<1$ kpc and up to $R \simeq 19$ kpc, we investigate the accuracy of
MOND and $\Lambda$CDM frameworks in addition to previously studied models, such
as the classical one with a Navarro-Frenk-White dark matter halo and a general
relativistic model. We find that all models, including MOND and $\Lambda$CDM,
are statistically equivalent in representing the observed rotational
velocities. However, $\Lambda$CDM, characterized by an Einasto density profile
and cosmological constraints on its parameters, assigns more dark matter than
the model featuring a Navarro-Frenk-White profile, with the virial mass
estimated at $1.5\text{-}2.5 \times 10^{12} \, {\rm M}_{\odot}$ - a value
significantly higher than recent literature estimates. Beyond $10\text{-}15$
kpc, non-Newtonian/non-baryonic contributions to the rotation curve are found
to become dominant for all models consistently. Our results suggest the need
for further exploration into the role of General Relativity, dark matter, and
alternative theories of gravitational dynamics in shaping Milky Way's rotation
curve.
