The mass and redshift of a cluster are its most fundamental properties. Linking observation to theory, these quantities allow us to use the evolution of cluster population over cosmic time to test models of structure formation. The dynamical state is a third, somewhat under-appreciated, fundamental quantity, affecting both clyster detectability in various surveys and our ability to reconstruct the mass. In this talk I will give a short overview of cluster mass estimation methods and the link between the radial mass distribution and the dynamical state. I will also address the prospects for measurement of the mass and dynamical state into the proto-cluster regime.