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(Abridged) From photometric observations of $\sim$ 47,000 stars andspectroscopy of $\sim$ 11,000 stars, we describe the first extensive study ofthe stellar population of the famous Double Cluster, h and $\chi$ Persei, downto subsolar masses. Both clusters have E(B-V) $\sim$ 0.52--0.55 and dM =11.8--11.85; the halo population, while more poorly constrained, likely hasidentical properties. As determined from the main sequence turnoff, theluminosity of M supergiants, and pre-main sequence isochrones, ages for hPersei, $\chi$ Persei and the halo population all converge on $\approx$ 14 Myr.  From these data, we establish the first spectroscopic and photometricmembership lists of cluster stars down to early/mid M dwarfs. At minimum, thereare $\sim$ 5,000 members within 10' of the cluster centers, while the entire hand $\chi$ Persei region has at least $\sim$ 13,000 and as many as 20,000members. The Double Cluster contains $\approx$ 8,400 M$_{\odot}$ of starswithin 10' of the cluster centers. We estimate a total mass of at least 20,000M$_{\odot}$. We conclude our study by outlining outstanding questions regardingthe properties of h and $\chi$ Persei. From comparing recent work, we compile alist of intrinsic colors and derive a new effective temperature scale for O--Mdwarfs, giants, and supergiants.

The Stellar Population of h and chi Persei: Cluster Properties, Membership, and the Intrinsic Colors and Temperatures of Stars