  With the start of JWST observations, mid-infrared (MIR) emission features
from polycyclic aromatic hydrocarbons (PAHs), H$_2$ rotational lines,
fine-structure lines from ions, and dust continuum will be widely available
tracers of gas and star formation rate (SFR) in galaxies at various redshifts.
Many of these tracers originate from dust and gas illuminated by UV photons
from massive stars, so they generally trace both SFR and gas to varying
degrees. We investigate how MIR spectral features from 5 to 35$\mu$m and
photometry from 3.4 to 250$\mu$m correlate with SFR traced by ionized neon
(15.6$\mu$m [Ne III] and 12.8$\mu$m [Ne II]) and molecular gas traced by carbon
monoxide (CO). In general, we find MIR emission features (i.e. PAHs and H$_2$
rotational lines) trace both CO and SFR better than CO and SFR trace one
another. H$_2$ lines and PAH features correlate best with CO. Fine-structure
lines from ions correlate best with SFR. The [S III] lines at 18.7 and
33.5$\mu$m, in particular, have a very tight correlation with SFR, and we use
them to calibrate new single-parameter MIR tracers of SFR that have negligible
metallicity dependence. The 17$\mu$m/7.7$\mu$m PAH feature ratio increases as a
function of CO emission which may be evidence of PAH growth or neutralization
in molecular gas. The degree to which dust continuum emission traces SFR or CO
varies as a function of wavelength, with continuum between 20 to 70$\mu$m
better tracing SFR, while longer wavelengths better trace CO.
