  Future space-based direct imaging missions will perform low-resolution
(R$<$100) optical (0.3-1~$\mu$m) spectroscopy of planets, thus enabling
reflected spectroscopy of cool giants. Reflected light spectroscopy is encoded
with rich information about the scattering and absorbing properties of planet
atmospheres. Given the diversity of clouds and hazes expected in exoplanets, it
is imperative we solidify the methodology to accurately and precisely retrieve
these scattering and absorbing properties that are agnostic to cloud species.
In particular, we focus on determining how different cloud parameterizations
affect resultant inferences of both cloud and atmospheric composition. We
simulate mock observations of the reflected spectra from three top priority
direct imaging cool giant targets with different effective temperatures,
ranging from 135 K to 533 K. We perform retrievals of cloud structure and
molecular abundances on these three planets using four different
parameterizations, each with increasing levels of cloud complexity. We find
that the retrieved atmospheric and scattering properties strongly depend on the
choice of cloud parameterization. For example, parameterizations that are too
simplistic tend to overestimate the abundances. Overall, we are unable to
retrieve precise/accurate gravity beyond $\pm$50\%. Lastly, we find that even
low SNR=5, low R=40 reflected light spectroscopy gives cursory zeroth order
insights into cloud deck position relative to molecular and Rayleigh optical
depth level.
