  3D kinetic-scale turbulence is studied numerically in the regime where
electrons are strongly magnetized (the ratio of plasma species pressure to
magnetic pressure is $\beta_e=0.1$ for electrons and $\beta_i=1$ for ions).
Such a regime is relevant in the vicinity of the solar corona, the Earth's
magnetosheath, and other astrophysical systems. The simulations, performed
using the fluid-kinetic spectral plasma solver (SPS) code, demonstrate that the
turbulent cascade in such regimes can reach scales smaller than the electron
inertial scale, and results in the formation of electron-scale current sheets
(ESCS). Statistical analysis of the geometrical properties of the detected ESCS
is performed using an algorithm based on the medial axis transform. A typical
half-thickness of the current sheets is found to be on the order of electron
inertial length or below, while their half-length falls between the electron
and ion inertial length. The pressure-strain interaction, used as a measure of
energy dissipation, exhibits high intermittency, with the majority of the total
energy exchange occurring in current structures occupying approximately 20\% of
the total volume. Some of the current sheets corresponding to the largest
pressure-strain interaction are found to be associated with Alfv\'enic electron
jets and magnetic configurations typical of reconnection. These reconnection
candidates represent about $1$\% of all the current sheets identified.
