  Kepler-33 hosts five validated transiting planets ranging in period from 5 to
41 days. The planets are in nearly co-planar orbits and exhibit remarkably
similar (appropriately scaled) transit durations indicative of similar impact
parameters. The outer three planets have radii of $3.5\lesssim R_{\rm
p}/R_\oplus\lesssim4.7$ and are closely-packed dynamically, and thus transit
timing variations can be observed. Photodynamical analysis of transit timing
variations provide $2\sigma$ upper bounds on the eccentricity of the orbiting
planets (ranging from $<0.02$ to $<0.2$) and the mean density of the host-star
($0.39_{-0.02}^{+0.01}\,{\rm g/cm^3}$). We combine \emph{Gaia} Early Data
Release 3 parallax observations, the previously reported host-star effective
temperature and metallicity, and our photodynamical model to refine properties
of the host-star and the transiting planets. Our analysis yields
well-constrained masses for Kepler-33~e ($6.6_{-1.0}^{+1.1}\,M_\oplus$) and f
($8.2_{-1.2}^{+1.6}\,M_\oplus$) along with $2\sigma$ upper limits for planets c
($<19\,M_\oplus$) and d ($<8.2\,M_\oplus$). We confirm the reported low bulk
densities of planet d ($<0.4\,{\rm g/cm^3}$), e ($0.8\pm0.1\,{\rm g/cm^3}$),
and f ($0.7\pm0.1\,{\rm g/cm^3}$). Based on comparisons with planetary
evolution models, we find that Kepler-33~e and f exhibit relatively high
envelope mass fractions of $f_{\rm env}=7.0_{-0.5}^{+0.6}\%$ and $f_{\rm
env}=10.3\pm0.6\%$, respectively. Assuming a mass for planet d
$\sim4\,M_\oplus$ suggests that it has $f_{\rm env}\gtrsim12\%$.
