  Observations of low-mass protostellar systems show evidence of rich complex
organic chemistry. Their low luminosity, however, makes determining abundance
distributions of complex organic molecules (COMs) within the water snowline
challenging. However, the excitation conditions sampled by differing molecular
distributions may produce substantive changes in the resulting emission. Thus,
molecular excitation may recover spatial information from spatially unresolved
data. By analyzing spatially-unresolved NOrthern Extended Millimeter Array
(NOEMA) observations of CH$_3$OH and CH$_3$CN, we aim to determine if CH$_3$OH
and CH$_3$CN are distributed differently in the protostellar disk around
HOPS-370, a highly-luminous intermediate mass protostar. Rotational diagram
analysis of CH$_3$OH and CH$_3$CN yields rotational temperatures of $198 \pm
1.2$ K and $448 \pm 19$ K, respectively, suggesting the two molecules have
different spatial distributions. Source-specific 3D LTE radiative transfer
models are used to constrain the spatial distribution of CH$_3$OH and CH$_3$CN
within the disk. A uniform distribution with an abundance of $4\times10^{-8}$
reproduces the CH$_3$OH observations. In contrast, the spatial distribution of
CH$_3$CN needs to be either more compact (within $\sim120$ au versus $\sim240$
au for CH$_3$OH) or exhibiting a factor of $\gtrsim 15$ increase in abundance
in the inner $\sim55$ au. A possible explanation for the difference in spatial
abundance distributions of CH$_3$OH and CH$_3$CN is carbon-grain sublimation.
