  We leverage recent numerical simulations of highly resolved star-forming
regions in a Milky Way-like Galaxy to explore the nature of extended gaseous
envelopes around molecular clouds. We extract a sample of two dozen
star-forming clouds from the feedback-dominated suite of the "Cloud Factory''
simulations. With the goal of exploring the 3D thermal and chemical structure
of the gas, we measure and fit the clouds' radial profiles in multiple tracers,
including $n_{H_I}$, $n_{H_2}$, $n_{H_{tot}}$, $n_{CO}$, and gas temperature.
We find that while solar neighborhood clouds recently detected via 3D dust
mapping have radially symmetric, low-density envelopes that extend $\sim$ 10-15
pc, the simulated cloud envelopes are primarily radially asymmetric with
low-density envelopes that extend only $\sim$ 2-3 pc. One potential explanation
for the absence of extended envelopes in the simulated clouds may be the lack
of magnetic fields, while a stronger local feedback prescription compared to
solar neighborhood conditions may drive the radially asymmetric cloud
morphologies. We make the pipeline to extract and characterize the radial
profile of clouds publicly available, which can be used in complementary and
future simulations to shed additional light on the key physics shaping the
formation and evolution of star-forming structures in the Milky Way.
