Clusters are one of the corner stones of cosmological parameter estimation from the Dark Energy Survey (DES). As shown by Rykoff et al. 2016, DES will detect thousands of clusters with well-measured redshifts and galaxy memberships. In order to realize the potential of these DES clusters for cosmology, it is essential that the scaling between galaxy membership and underlying halo mass is measured. This includes not only the slope of the scaling, but its normalization, scatter, and the evolution of those parameters. Halo mass is not a directly observable parameter, so DES is using proxies such as weak lensing, the Sunyaev Zeldovich effect, X-ray luminosity and X-ray temperature. In Rykoff et al. (2016) we presented an X-ray to optical scaling analysis presented in based on 200 sq.degrees of Science Verification observations, which overlapped ~30 XMM observations of clusters. In this talk , we will present results from more than 10x that area/number.