  We present results from the first 3D kinetic numerical simulation of
magnetorotational turbulence and dynamo, using the local shearing-box model of
a collisionless accretion disc. The kinetic magnetorotational instability grows
from a subthermal magnetic field having zero net flux over the computational
domain to generate self-sustained turbulence and outward angular-momentum
transport. Significant Maxwell and Reynolds stresses are accompanied by
comparable viscous stresses produced by field-aligned ion pressure anisotropy,
which is regulated primarily by the mirror and ion-cyclotron instabilities
through particle trapping and pitch-angle scattering. The latter endow the
plasma with an effective viscosity that is biased with respect to the
magnetic-field direction and spatio-temporally variable. Energy spectra suggest
an Alfv\'en-wave cascade at large scales and a kinetic-Alfv\'en-wave cascade at
small scales, with strong small-scale density fluctuations and weak
non-axisymmetric density waves. Ions undergo non-thermal particle acceleration,
their distribution accurately described by a kappa distribution. These results
have implications for the properties of low-collisionality accretion flows,
such as that near the black hole at the Galactic center.
