For several decades X-ray instruments have provided us with spectral and imaging data of solar flares, however a key diagnostic has been missing: the electron angular distribution. The angular distribution (or directivity) of electrons provides insight into the acceleration mechanism as well as the role of transport effects, and can be determined from hard X-ray directivity. Here, we use kinetic modeling to describe the acceleration and transport of flare electrons. We produce outputs for the density-weighted electron flux, a quantity directly related to observed X-rays. From these outputs we consider how the electron angular distribution changes in energy and space across a solar flare by studying the electron pitch angle distribution. We explore two extremes of electrons being scattered from turbulence: (1) when there is no turbulent scattering (2) very frequent scattering. We find, during case 1 electrons may get trapped in the acceleration region moving perpendicular to the magnetic field, gaining energy continuously and forming a pancake-shaped pitch angle distribution. In case 2 electrons are scattered so frequently they cannot leave the acceleration region, becoming trapped, and gaining energy, producing an angular distribution that is aligned with the magnetic field.