  We numerically calculate the evolution of second order cosmological
perturbations for an inflationary scalar field without resorting to the
slow-roll approximation or assuming large scales. In contrast to previous
approaches we therefore use the full non-slow-roll source term for the second
order Klein-Gordon equation which is valid on all scales. The numerical results
are consistent with the ones obtained previously where slow-roll is a good
approximation. We investigate the effect of localised features in the scalar
field potential which break slow-roll for some portion of the evolution. The
numerical package solving the second order Klein-Gordon equation has been
released under an open source license and is available for download.
