Planet forming disks are ubiquitous, naturally produced via the collapse of angular momentum bearing protostellar clouds. While many observational efforts have focused on later stage dusty protoplanetary systems, recent surveys of star forming regions have suggested that planet formation may be occurring much earlier. Understanding the physics of the earlier embedded systems is then crucial for characterizing protoplanetary disks and the conditions for planet formation. I will present results from a series of large scale numerical studies that produce statistical distributions of protostellar properties. I will show how these properties, inherited from the star forming environment, give rise to the initial conditions for disk formation and discuss what will be required to construct realistic models of embedded objects.