  The degree to which the thin accretion disks of black hole X-ray binaries are
truncated during hard spectral states remains a contentious open question in
black hole astrophysics. During its singular observed outburst in
$2009\mbox{--}2010$, the black hole X-ray binary XTE J1752-223 spent
$\sim1$~month in a long-stable hard spectral state at a luminosity of
$\sim0.02\mbox{--}0.1~L_{\rm Edd}$. It was observed with 56 RXTE pointings
during this period, with simultaneous Swift-XRT daily coverage during the first
10 days of the RXTE observations. Whilst reflection modeling has been
extensively explored in the analysis of these data, there is a disagreement
surrounding the geometry of the accretion disk and corona implied by the
reflection features. We re-examine the combined, high signal-to-noise,
simultaneous Swift and RXTE observations, and perform extensive reflection
modeling with the latest relxill suite of reflection models, including newer
high disk density models. We show that reflection modeling requires that the
disk be within $\sim5~R_{\rm ISCO}$ during the hard spectral state, whilst
weaker constraints from the thermal disk emission imply higher truncation
($R_{\rm in}=6\mbox{--}80~R_{\rm ISCO}$). We also explore more complex coronal
continuum models, allowing for two Comptonization components instead of one,
and show that the reflection features still require only a mildly truncated
disk. Finally we present a full comparison of our results to previous
constraints found from analyses of the same dataset.
