  We report high-resolution, high-cadence observations of five small-scale
coronal jets in an on-disk quiet Sun region observed with Solar Orbiter's
EUI/\hri\ in 174 \AA. We combine the \hri\ images with the EUV images of
SDO/AIA and investigate magnetic setting of the jets using co-aligned
line-of-sight magnetograms from SDO/HMI. The \hri\ jets are miniature versions
of typical coronal jets as they show narrow collimated spires with a base
brightening. Three out of five jets result from a detectable minifilament
eruption following flux cancelation at the neutral line under the minifilament,
analogous to coronal jets. To better understand the physics of jets, we also
analyze five small-scale jets from a high-resolution Bifrost MHD simulation in
synthetic \FeIX/\FeX\ emissions. The jets in the simulation reside above
neutral lines and four out of five jets are triggered by magnetic flux
cancelation. The temperature maps show the evidence of cool gas in the same
four jets. Our simulation also shows the signatures of opposite Doppler shifts
(of the order of $\pm$10s of \kms) in the jet spire, which is evidence of
untwisting motion of the magnetic field in the jet spire. The average jet
duration, spire length, base width, and speed in our observations (and in
synthetic \FeIX/\FeX\ images) are 6.5$\pm$4.0 min (9.0$\pm$4.0 min),
6050$\pm$2900 km (6500$\pm$6500 km), 2200$\pm$850 km, (3900$\pm$2100 km), and
60$\pm$8 \kms\ (42$\pm$20 \kms), respectively. Our observation and simulation
results provide a unified picture of small-scale solar coronal jets driven by
magnetic reconnection accompanying flux cancelation. This picture also aligns
well with the most recent reports of the formation and eruption mechanisms of
larger coronal jets.
