  As a relatively young and bright population, and the archetype of standard
candles, classical Cepheids make an ideal population to trace non-axisymmetric
structure in the young stellar disk to large distances. We use the new
distances derived in Paper I based on mid-IR WISE photometry for a selected
sample of 2857 dynamically young Cepheids to trace the spiral arms of the Milky
Way. The Perseus and Sagittarius-Carina arms are clearly evident in the third
and fourth Galactic quadrants, while the Local and Scutum arms are much weaker,
with extinction severely limiting our view of the latter, inner-most spiral
arm. Pitch angles are derived for each arm over various ranges of galactic
azimuth, each covering at least 90{\deg} in azimuth. Our method of detecting
spiral arms and deriving pitch angles does not rely on pre-assigning sources to
specific arms. While spiral structure in the first and second quadrant is not
obvious, in part due to extinction effects, it is not inconsistent with that
seen in the third and fourth quadrants. In summary, the Cepheids allow us to
map spiral structure in the third and fourth Galactic quadrants where there are
currently few masers with astrometric parallaxes, thus significantly extending
our picture of the Milky Way on large-scales.
