  The majority of existing results for the kilonova (or macronova) emission
from material ejected during a neutron-star (NS) merger is based on
(quasi-)one-zone models or manually constructed toy-model ejecta
configurations. In this study we present a kilonova analysis of the material
ejected during the first ~10ms of a NS merger, called dynamical ejecta, using
directly the outflow trajectories from general relativistic smoothed-particle
hydrodynamics simulations including a sophisticated neutrino treatment and the
corresponding nucleosynthesis results, which have been presented in Part I of
this study. We employ a multi-dimensional two-moment radiation transport scheme
with approximate M1 closure to evolve the photon field and use a heuristic
prescription for the opacities found by calibration with atomic-physics based
reference results. We find that the photosphere is generically ellipsoidal but
augmented with small-scale structure and produces emission that is about 1.5-3
times stronger towards the pole than the equator. The kilonova typically peaks
after 0.7-1.5days in the near-infrared frequency regime with luminosities
between 3-7x10^40erg/s and at photospheric temperatures of 2.2-2.8x10^3K. A
softer equation of state or higher binary-mass asymmetry leads to a longer and
brighter signal. Significant variations of the light curve are also obtained
for models with artificially modified electron fractions, emphasizing the
importance of a reliable neutrino-transport modeling. None of the models
investigated here, which only consider dynamical ejecta, produces a transient
as bright as AT2017gfo. The near-infrared peak of our models is incompatible
with the early blue component of AT2017gfo.
