  We investigate the initiation of cosmic inflation, in full numerical
relativity, from pre-inflationary scenarios with large tensor and vector
fluctuations in the metric. These settings are characterized by having large
values in the Weyl curvature tensor. In the matter sector, we consider a single
scalar field with inhomogeneous field velocities, corresponding to a kination
period. In the context of large-field inflation, it is shown that the onset of
inflation continues to be robust to this type of initial conditions, and that
during inflation the Universe successfully homogenizes and flattens any type of
curvature, leading to a Friedmann-Lema\^itre-Robertson-Walker Universe after
just a few tens of efolds of accelerating expansion.
