  We use high-resolution cosmological zoom simulations with ~200 pc resolution
at z = 2 and various prescriptions for galactic outflows in order to explore
the impact of winds on the morphological, dynamical, and structural properties
of eight individual galaxies with halo masses ~ 10^11--2x10^12 Msun at z = 2.
We present a detailed comparison to spatially and spectrally resolved H{\alpha}
and other observations of z ~ 2 galaxies. We find that simulations without
winds produce massive, compact galaxies with low gas fractions, super-solar
metallicities, high bulge fractions, and much of the star formation
concentrated within the inner kpc. Strong winds are required to maintain high
gas fractions, redistribute star-forming gas over larger scales, and increase
the velocity dispersion of simulated galaxies, more in agreement with the
large, extended, turbulent disks typical of high-redshift star-forming
galaxies. Winds also suppress early star formation to produce high-redshift
cosmic star formation efficiencies in better agreement with observations.
Sizes, rotation velocities, and velocity dispersions all scale with stellar
mass in accord with observations. Our simulations produce a diversity of
morphological characteristics - among our three most massive galaxies, we find
a quiescent grand-design spiral, a very compact star-forming galaxy, and a
clumpy disk undergoing a minor merger; the clumps are evident in H{\alpha} but
not in the stars. Rotation curves are generally slowly rising, particularly
when calculated using azimuthal velocities rather than enclosed mass. Our
results are broadly resolution-converged. These results show that cosmological
simulations including outflows can produce disk galaxies similar to those
observed during the peak epoch of cosmic galaxy growth.
