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We report on the presence of numerous tiny bright dots in and around anemerging flux region (an X-ray/coronal bright point) observed with SolO'sEUI/\hri\ in 174 \AA. These dots are roundish, have a diameter of 675$\pm$300km, a lifetime of 50$\pm$35 seconds, and an intensity enhancement of 30\%$\pm$10\% above their immediate surroundings. About half of the dots remainisolated during their evolution and move randomly and slowly ($<$10 \kms). Theother half show extensions, appearing as a small loop or surge/jet, withintensity propagations below 30\,\kms. Many of the bigger and brighter \hri\dots are discernible in SDO/AIA 171 \AA\ channel, have significant emissivityin the temperature range of 1--2 MK, and are often located at polarityinversion lines observed in HMI LOS magnetograms. Although not as pervasive asin observations, Bifrost MHD simulation of an emerging flux region do show dotsin synthetic \fe\ images. These dots in simulation show distinct Dopplersignatures -- blueshifts and redshifts coexist, or a redshift of the order of10 \kms\ is followed by a blueshift of similar or higher magnitude. Thesynthetic images of \oxy\ and \siiv\ lines, which represent transition regionradiation, also show the dots that are observed in \fe\ images, often expandedin size, or extended as a loop, and always with stronger Doppler velocities (upto 100 \kms) than that in \fe\ lines. Our observation and simulation results,together with the field geometry of dots in the simulation, suggest that mostdots in emerging flux regions form in the lower solar atmosphere (at $\approx$1Mm) by magnetic reconnection between emerging and pre-existing/emerged magneticfield. Some dots might be manifestations of magneto-acoustic shocks through theline formation region of \fe\ emission.

SolO/EUI Observations of Ubiquitous Fine-scale Bright Dots in an Emerging Flux Region: Comparison with a Bifrost MHD Simulation