We have performed an extremely high resolution numerical simulation of the Moon-forming impact using a well-tested SPH (Smoothed Particle Hydrodynamics) code with 10^8 particles within the simulation domain. SPH codes are well-suited to computing gravitational interactions, tracking provenance, 3D geometry, extreme computational parallelization, and they are guaranteed to conserve matter. Furthermore, the time integration scheme is designed to approximately conserve energy and angular momentum. These qualities have made SPH codes the usual choice for this problem. Our simulation contains 100 times more particles than in the state-of-the-art simulations published to date, which typically deploy a few million particles (Canup 2004, Canup 2008, Reufer 2012, Cuk and Stewart 2012, Canup and Crawford 2013). This simulation has achieved spatial resolutions on the order of ~30 km in the planet and a few hundred kilometers in the moon-forming disk. These resolutions are approximately an order of magnitude finer than in any of the aforementioned published simulations. A careful reading of a very recent study of resolution-dependence of Moon-forming impact simulations (Canup and Crawford 2013) shows that at least two important constraints on impact outcomes — the iron content of the Moon-forming disk and the amount of material with orbits lying wholly beyond the Roche limit — have not converged to stable limits in 10^6 particle simulations (nor in Eulerian simulations of comparable spatial resolution). Higher resolution is required to address these issues by (i) vertically resolving the disk, and (ii) reducing numerical viscosity into the estimated range of physical viscosities. We have applied very well tested algorithms used in Cosmology to find bound objects within the moon-forming impact disk to produce the mass function of these `moonlets' at different times. This will shed light on the temporal evolution of the Moon-forming disk sub-structure and the eventual fate of such objects. Earlier work, with lower resolution simulations, suggests that these bound objects are short lived while our high resolution simulation seems to show that these substructures can survive for most of the Moon-forming disk history.