  Sheath regions of interplanetary coronal mass ejections (ICMEs) are formed
when the upstream solar wind is deflected and compressed due to the propagation
and expansion of the ICME. Small-scale flux ropes found in the solar wind can
thus be swept into ICME-driven sheath regions. They may also be generated
locally within the sheaths through a range of processes. This work applies
wavelet analysis to obtain the normalized reduced magnetic helicity, normalized
cross helicity, and normalized residual energy, and uses them to identify
small-scale flux ropes and Alfv\'en waves in 55 ICME-driven sheath regions
observed by the Wind spacecraft in the near-Earth solar wind. Their occurrence
is investigated separately for three different frequency ranges between
$10^{-2} - 10^{-4}$ Hz. We find that small scale flux ropes are more common in
ICME sheaths than in the upstream wind, implying that they are at least to some
extent actively generated in the sheath and not just compressed from the
upstream wind. Alfv\'en waves occur more evenly in the upstream wind and in the
sheath. This study also reveals that while the highest frequency (smallest
scale) flux ropes occur relatively evenly across the sheath, the lower
frequency (largest scale) flux ropes peak near the ICME leading edge. This
suggests that they could have different physical origins, and that processes
near the ICME leading edge are important for generating the larger scale
population.
