  The structural parameters of a galaxy can be used to gain insight into its
formation and evolution history. In this paper, we strive to compare the Milky
Way's structural parameters to other, primarily edge-on, spiral galaxies in
order to determine how our Galaxy measures up to the Local Universe. For our
comparison, we use the galaxy structural parameters gathered from a variety of
literature sources in the optical and near-infrared wavebands. We compare the
scale length, scale height, and disk flatness for both the thin and thick
disks, the thick-to-thin disk mass ratio, the bulge-to-total luminosity ratio,
and the mean pitch angle of the Milky Way's spiral arms to those in other
galaxies. We conclude that many of the Milky Way's structural parameters are
largely ordinary and typical of spiral galaxies in the Local Universe, though
the Galaxy's thick disk appears to be appreciably thinner and less extended
than expected from zoom-in cosmological simulations of Milky Way-mass galaxies
with a significant contribution of galaxy mergers involving satellite galaxies.
