  Measurements of short-timescale star formation variations (i.e.,
"burstiness") are integral to our understanding of star formation feedback
mechanisms and the assembly of stellar populations in galaxies. We expand upon
the work of Broussard et al. (2019) by introducing a new analysis of galaxy
star formation burstiness that accounts for variations in the
$Q_{sg}=\mathrm{E(B-V)_{stars}}/\mathrm{E(B-V)_{gas}}$ distribution, a major
confounding factor. We use Balmer decrements from the MOSFIRE Deep Evolution
Field (MOSDEF) survey to measure $Q_{sg}$, which we use to construct mock
catalogs from the Santa Cruz Semi-Analytic Models and Mufasa cosmological
hydrodynamical simulation based on 3D-HST, Fiber Multi-Object Spectrograph
(FMOS)-COSMOS, and MOSDEF galaxies with H$\alpha$ detections. The results of
the mock catalogs are compared against observations using the burst indicator
$\eta = \log_{10}(\mathrm{SFR_{H\alpha}/SFR_{NUV}})$, with the standard
deviation of the $\eta$ distribution indicating burstiness. We find decent
agreement between mock and observed $\eta$ distribution shapes; however, the
FMOS-COSMOS and MOSDEF mocks show a systematically low median and scatter in
$\eta$ in comparison to the observations. This work also presents the novel
approach of analytically deriving the relationship between the intrinsic
scatter in $\eta$, scatter added by measurement uncertainties, and observed
scatter, resulting in an intrinsic burstiness measurement of $0.06-0.16$ dex.
