  JWST will provide moderate resolution transit spectra with continuous
wavelength coverage from the optical to the mid-infrared for the first time. In
this paper, we illustrate how different aerosol species, size-distributions,
and spatial distributions encode information in JWST transit spectra. We use
the transit spectral modeling code METIS, along with Mie theory and several
flexible treatments of aerosol size and spatial distributions to perform
parameter sensitivity studies, calculate transit contribution functions,
compute Jacobians, and retrieve parameters with Markov Chain Monte Carlo. The
broader wavelength coverage of JWST will likely encompass enough non-gray
aerosol behavior to recover information about the species and size-distribution
of particles, especially if distinct resonance features arising from the
aerosols are present. Within the JWST wavelength range, the optical and
mid-infrared typically provide information about 0.1-1 $\mu$m sized aerosols,
while the near-infrared to mid-infrared wavelengths usually provide information
about gaseous absorption, even if aerosols are present. Strong gaseous
absorption features in the infrared often remain visible, even when clouds and
hazes are flattening the optical and NIR portion of the spectrum that is
currently observable. For some combinations of aerosol properties, temperature,
and surface gravity, one can make a precise measure of metallicity despite the
presence of aerosols, but more often the retrieved metallicity of a cloudy or
hazy atmosphere has significantly lower precision than for a clear atmosphere
with otherwise similar properties. Future efforts to securely link aerosol
properties to atmospheric metallicity and temperature in a physically motivated
manner will ultimately enable a robust physical understanding of the processes
at play in cloudy, hazy exoplanet atmospheres.
