The influence on ion motion of magnetic turbulence observed in the near-Earth magnetotail is investigated by numerical simulation. The magnetotail current sheet is modeled as a magnetic field reversal with a normal magnetic field component Bn, plus a three-dimensional spectrum of magnetic fluctuations δB, which represents the observed magnetic turbulence. A cross tail electric field Ey is included. A test particle simulation is performed assuming an anisotropic plasma source at the magnetospheric lobes, and using different values of Bn and of the fluctuation level δB/B0. In the relevant range of parameters, Bn and δB/B0 have opposite effects on the current structure and on the ion heating. In particular, for a substantial level of fluctuations, δB/B0 ≳ 0.2, the current splits into two sheets for Bn ~ 0, but increasing Bn requires a higher δB/B0 in order to have the current splitting. In addition, ion heating increases with the increase of δB/B0 and with the decrease of Bn, as these changes favor motion perpendicular to the average magnetic field and along the potential drop. When the magnetic fluctuations are small, the diamagnetic current wings and the magnetic field overshoots at the boundary of the current sheet are recovered for weakly anisotropic plasma distributions. Implications for the substorm growth phase and onset are discussed.