  We investigate the fine-structure [C${\rm \scriptsize II}$] line at
$158\,\mu$m as a molecular gas tracer by analyzing the relationship between
molecular gas mass ($M_{\rm mol}$) and [C${\rm \scriptsize II}$] line
luminosity ($L_{\rm [CII]}$) in 11,125 $z\simeq 6$ star-forming, main sequence
galaxies from the SIMBA simulations, with line emission modeled by S\'IGAME.
Though most ($\sim 50-100\,\%$) of the gas mass in our simulations is ionized,
the bulk ($> 50\,\%$) of the [C${\rm \scriptsize II}$] emission comes from the
molecular phase. We find a sub-linear (slope $0.78\pm 0.01$) $\log L_{\rm
[CII]}-\log M_{\rm mol}$ relation, in contrast with the linear relation derived
from observational samples of more massive, metal-rich galaxies at $z \lesssim
6$. We derive a median [C${\rm \scriptsize II}$]-to-$M_{\rm mol}$ conversion
factor of $\alpha_{\rm [CII]} \simeq 18\,{\rm M_{\rm \odot}/L_{\rm \odot}}$.
This is lower than the average value of $\simeq 30\,{\rm M_{\rm \odot}/L_{\rm
\odot}}$ derived from observations, which we attribute to lower gas-phase
metallicities in our simulations. Thus, a lower, luminosity-dependent,
conversion factor must be applied when inferring molecular gas masses from
[C${\rm \scriptsize II}$] observations of low-mass galaxies. For our
simulations, [C${\rm \scriptsize II}$] is a better tracer of the molecular gas
than CO $J=1-0$, especially at the lowest metallicities, where much of the gas
is 'CO-dark'. We find that $L_{\rm [CII]}$ is more tightly correlated with
$M_{\rm mol}$ than with star-formation rate (${\rm SFR}$), and both the $\log
L_{\rm [CII]}-\log M_{\rm mol}$ and $\log L_{\rm [CII]}-\log {\rm SFR}$
relations arise from the Kennicutt-Schmidt relation. Our findings suggest that
$L_{\rm [CII]}$ is a promising tracer of the molecular gas at the earliest
cosmic epochs.
