  We present ALMA observations of the dwarf starburst galaxy Henize 2-10 in
combination with previous SMA CO observations to probe the molecular
environments of natal super star clusters. These observations include the
HCO$^+$(1-0), HCN(1-0), HNC(1-0), and CCH(1-0) molecular lines, as well as 88
GHz continuum with a spatial resolution of $1''.7\times 1''.6$. After
correcting for the contribution from free-free emission to the 88 GHz continuum
flux density ($\sim$ 60% of the 88 GHz emission), we derive a total gas mass
for He~2-10 of $M_{gas} = 4-6\times10^8$ M$_{\odot}$, roughly 5-20% of the
dynamical mass. Based on a principle component analysis, HCO$^+$ is found to be
the best "general" tracer of molecular emission. The line widths and
luminosities of the CO emission suggests that the molecular clouds could either
be as small as $\sim 8$ pc, or alternately have enhanced line widths. The CO
emission and 88 GHz continuum are anti-correlated, suggesting that either the
dust and molecular gas are not cospatial, which could reflect the 88 GHz
continuum is dominated by free-free emission. The CO and CCH emission are also
relatively anti-correlated, which is consistent with the CCH being
photo-enhanced, and/or the CO being dissociated in the regions near the natal
super star clusters. The molecular line ratios of regions containing the natal
star clusters are different from the line ratios observed for regions elsewhere
in the galaxy. In particular, the regions with thermal radio emission all have
CO(2-1)/HCO$^+(1-0) < 16$, and the HCO$^+$/CO ratio appears to be correlated
with the evolutionary stage of the clusters.
