  We use the adaptive mesh refinement code RAMSES to model the formation of
protoplanetary disks in realistic star formation environments. The resolution
scales over up to 29 powers of two ($\sim$ 9 orders of magnitude) covering a
range from outer scales of 40 pc to inner scales of 0.015 AU. The accretion
rate from a 1.5 solar mass envelope peaks near $10^{-4}$ $\mspy$ about 6 kyr
after sink particle formation and then decays approximately exponentially,
reaching $10^{-6}$ $\mspy$ in 100 kyr. The models suggest universal scalings of
physical properties with radius during the main accretion phase, with kinetic
and / or magnetic energy in approximate balance with gravitational energy.
Efficient accretion is made possible by the braking action of the magnetic
field, which nevertheless allows a near-Keplerian disk to grow to a 100 AU
size. The magnetic field strength ranges from more than 10 G at 0.1 AU to less
than 1 mG at 100 AU, and drives a time dependent bipolar outflow, with a
collimated jet and a broader disk wind.
