  We report on the presence of numerous tiny bright dots in and around an
emerging flux region (an X-ray/coronal bright point) observed with SolO's
EUI/\hri\ in 174 \AA. These dots are roundish, have a diameter of 675$\pm$300
km, a lifetime of 50$\pm$35 seconds, and an intensity enhancement of 30\%
$\pm$10\% above their immediate surroundings. About half of the dots remain
isolated during their evolution and move randomly and slowly ($<$10 \kms). The
other half show extensions, appearing as a small loop or surge/jet, with
intensity propagations below 30\,\kms. Many of the bigger and brighter \hri\
dots are discernible in SDO/AIA 171 \AA\ channel, have significant emissivity
in the temperature range of 1--2 MK, and are often located at polarity
inversion lines observed in HMI LOS magnetograms. Although not as pervasive as
in observations, Bifrost MHD simulation of an emerging flux region do show dots
in synthetic \fe\ images. These dots in simulation show distinct Doppler
signatures -- blueshifts and redshifts coexist, or a redshift of the order of
10 \kms\ is followed by a blueshift of similar or higher magnitude. The
synthetic images of \oxy\ and \siiv\ lines, which represent transition region
radiation, also show the dots that are observed in \fe\ images, often expanded
in size, or extended as a loop, and always with stronger Doppler velocities (up
to 100 \kms) than that in \fe\ lines. Our observation and simulation results,
together with the field geometry of dots in the simulation, suggest that most
dots in emerging flux regions form in the lower solar atmosphere (at $\approx$1
Mm) by magnetic reconnection between emerging and pre-existing/emerged magnetic
field. Some dots might be manifestations of magneto-acoustic shocks through the
line formation region of \fe\ emission.
