  The Small Magellanic Cloud (SMC) provides the only laboratory to study the
structure of molecular gas at high resolution and low metallicity. We present
results from the Herschel Spectroscopic Survey of the SMC (HS$^{3}$), which
mapped the key far-IR cooling lines [CII], [OI], [NII], and [OIII] in five
star-forming regions, and new ALMA 7m-array maps of $^{12}$CO and $^{13}$CO
$(2-1)$ with coverage overlapping four of the five HS$^{3}$ regions. We detect
[CII] and [OI] throughout all of the regions mapped. The data allow us to
compare the structure of the molecular clouds and surrounding photodissociation
regions using $^{13}$CO, CO, [CII], and [OI] emission at $<10$" ($<3$ pc)
scales. We estimate Av using far-IR thermal continuum emission from dust and
find the CO/[CII] ratios reach the Milky Way value at high A$_{V}$ in the
centers of the clouds and fall to $\sim{1/5-1/10}\times$ the Milky Way value in
the outskirts, indicating the presence of translucent molecular gas not traced
by bright CO emission. We estimate the amount of molecular gas traced by bright
[CII] emission at low A$_{V}$ and bright CO emission at high A$_{V}$. We find
that most of the molecular gas is at low A$_{V}$ and traced by bright [CII]
emission, but that faint CO emission appears to extend to where we estimate the
H$_{2}$-to-HI transition occurs. By converting our H$_{2}$ gas estimates to a
CO-to-H$_{2}$ conversion factor ($X_{CO}$), we show that $X_{CO}$ is primarily
a function of A$_{V}$, consistent with simulations and models of low
metallicity molecular clouds.
