  Decayless kink oscillations are omnipresent in the solar atmosphere and a
viable candidate for coronal heating. Though there have been extensive studies
of decayless oscillations in coronal loops with a few hundred Mm lengths, the
properties of these oscillations in small-scale ($\sim$10 Mm) loops are yet to
be explored. In this study, we present the properties of decayless oscillations
in small loops embedded in the quiet corona and coronal holes. We use high
resolution observations from the Extreme Ultraviolet Imager onboard Solar
Orbiter with pixel scales of 210 km and 5 s cadence or better. We find 42
oscillations in 33 coronal loops with loop lengths varying between 3 to 23 Mm.
The average displacement amplitude is found to be 136 km. The oscillations
period has a range of 27 to 276 s, and the velocity amplitudes range from 2.2
to 19.3 km s$^{-1}$. The observed kink speeds are lower than those observed in
active region coronal loops. The variation of loop length with the period does
not indicate a strong correlation. Coronal seismology technique indicated an
average magnetic field value of 2.1 G. We estimate the energy flux with a broad
range of 0.6-314 W m$^{-2}$. Moreover, we note that the short-period decayless
oscillations are not prevalent in the quiet Sun and coronal holes. Therefore,
our study suggests that decayless oscillations in small-scale coronal loops are
unlikely to provide enough energy to heat the quiet Sun and accelerate solar
wind in the coronal holes.
