  Hydrodynamic simulations of the stellar winds from Wolf-Rayet stars within
the Galactic Center can provide predictions for the X-ray spectrum of
supermassive black hole Sgr A*. Herein, we present results from updated smooth
particle hydrodynamics simulations, building on the architecture of Cuadra et
al. (2015); Russell et al. (2017), finding that a cold gas disk forms around
Sgr A* with a simulation runtime of 3500 years. This result is consistent with
previous grid-based simulations, demonstrating that a cold disk can form
regardless of numerical method. We examine the plasma scenarios arising from an
environment with and without this cold disk, by generating synthetic spectra
for comparison to the quiescent Fe K alpha Sgr A* spectrum from Chandra HETG-S,
taken through the Chandra X-ray Visionary Program. We find that current and
future X-ray missions are unlikely to distinguish between the kinematic
signatures in the plasma in these two scenarios. Nonetheless, the stellar wind
plasma model presents a good fit to the dispersed Chandra spectra within 1.5"
of Sgr A*. We compare our results to the Radiatively Inefficient Accretion Flow
(RIAF) model fit to the HETG-S spectrum presented in Paper I and find that the
Bayesian model evidence does not strongly favor either model. With 9" angular
resolution and high spectral resolution of the X-IFU, NewAthena will offer a
clearer differentiation between the RIAF plasma model and hydrodynamic
simulations, but only a future X-ray mission with arcsecond resolution will
significantly advance our understanding of Sgr A*'s accretion flow in X-rays.
