With the chronological resolution provided by the panoply of radioisotope chronometers now in use we have the ability to distinguish the various steps involved in planet growth to a degree where we can no longer think of a single age of formation, but instead a prolonged interval for growth and differentiation. As these chronometers date events that change the chemical composition of the object being analyzed, the three main processes in planet formation that can be precisely dated involve the separation of volatile from refractory elements, the metal-silicate separation that accompanies core formation, and often the differentiation of a global silicate magma ocean driven by the gravitational sorting of crystals from melt. This talk will explore these steps in Moon formation to reach the conclusion that the first two processes described above occurred not on the Moon but on the planets/planetesimals from which the Moon formed, and that data for crystallization of the lunar magma ocean suggest that the Moon did not exist as an isolated body until up to 150-200 Myr after the beginning of Solar System formation.