  We measured $^{35}$Cl abundances in 52 M giants with metallicities between
-0.5 $<$ [Fe/H] $<$ 0.12. Abundances and atmospheric parameters were derived
using infrared spectra from CSHELL on the IRTF and from optical echelle
spectra. We measured Cl abundances by fitting a H$^{35}$Cl molecular feature at
3.6985 $\mu$m with synthetic spectra. We also measured the abundances of O, Ca,
Ti, and Fe using atomic absorption lines. We find that the [Cl/Fe] ratio for
our stars agrees with chemical evolution models of Cl and the [Cl/Ca] ratio is
broadly consistent with the solar ratio over our metallicity range. Both
indicate that Cl is primarily made in core-collapse supernovae with some
contributions from Type Ia SN. We suggest other potential nucleosynthesis
processes, such as the $\nu$-process, are not significant producers of Cl.
Finally, we also find our Cl abundances are consistent with H II and planetary
nebular abundances at a given oxygen abundance, although there is scatter in
the data.
