  It has been shown in previous publications that the TNG100 simulation
quantitatively reproduces the observed reduction in each of the total atomic
and total molecular hydrogen gas for galaxies within massive halos, i.e.~dense
environments. In this Letter, we study how well TNG50 reproduces the resolved
effects of a Virgo-like cluster environment on the gas surface densities of
satellite galaxies with $m_* > \! 10^9\,{\rm M}_\odot$ and ${\rm SFR} \! >
0.05\,{\rm M}_\odot\,{\rm yr}^{-1}$. We select galaxies in the simulation that
are analogous to those in the HERACLES and VERTICO surveys, and mock-observe
them to the common specifications of the data. Although TNG50 does not
quantitatively match the observed gas surface densities in the centers of
galaxies, the simulation does qualitatively reproduce the trends of gas
truncation and central density suppression seen in VERTICO in both HI and
H$_2$. This result promises that modern cosmological hydrodynamic simulations
can be used to reliably model the post-infall histories of cluster satellite
galaxies.
