The dynamics and outcome of star formation with jets, radiation, winds,
  and supernovae in concert
  We analyze the first giant molecular cloud (GMC) simulation to follow the
formation of individual stars and their feedback from jets, radiation, winds,
and supernovae, using the STARFORGE framework in the GIZMO code. We evolve the
GMC for $\sim 9 \rm Myr$, from initial turbulent collapse to dispersal by
feedback. Protostellar jets dominate feedback momentum initially, but radiation
and winds cause cloud disruption at $\sim 8\%$ star formation efficiency (SFE),
and the first supernova at $8.3 \rm Myr$ comes too late to influence star
formation significantly. The per-freefall SFE is dynamic, accelerating from 0
to $\sim 18\%$ before dropping quickly to <1%, but the estimate from YSO counts
compresses it to a narrower range. The primary cluster forms hierarchically and
condenses to a brief ($\sim 1\,\mathrm{Myr}$) compact ($\sim 1 \rm pc$) phase,
but does not virialize before the cloud disperses, and the stars end as an
unbound expanding association. The initial mass function resembles the Chabrier
(2005) form with a high-mass slope $\alpha=-2$ and a maximum mass of $55
M_\odot$. Stellar accretion takes $\sim 400 \rm kyr$ on average, but $\gtrsim
1\rm Myr$ for $>10 M_\odot$ stars, so massive stars finish growing latest. The
fraction of stars in multiples increases as a function of primary mass, as
observed. Overall, the simulation much more closely resembles reality, compared
to variations which neglect different feedback physics entirely. But more
detailed comparison with synthetic observations is necessary to constrain the
theoretical uncertainties.
