  The small-scale moving intensity enhancements remotely observed in the
extreme ultraviolet images of the solar active regions, which we refer to as
active region moving campfires (ARMCs), are related to local plasma temperature
and/or density enhancements. Their dynamics is driven by the physical processes
in the entire coronal plasma. Our previous study of ARMCs indicates that they
have characteristic velocities at around the background sound speed. The main
goal of our work is to carry out a simultaneous analysis of EUV images from two
observational missions, SDO/AIA and Hi-C 2.1. The aims of the performed
cross-validating analysis of both SDO/AIA and Hi-C 2.1 data were to reveal how
the observed moving features are distributed over the studied active region,
AR12712, test the existence of different groups of ARMCs with distinct physical
characteristics. We use the statistical model of intensity centroid convergence
and tracking that was developed in our previous paper. Furthermore, a Gaussian
mixture model fit of the observed complex of moving ARMCs is elaborated to
reveal the existence of distinct ARMC groups and to study the physical
characteristics of these different groups. In data from the 171\AA, 193\AA\ and
211\AA\ channels of SDO/AIA, we identified several groups of ARMCs with respect
to both blob intensity and velocity profiles. The existence of such groups is
confirmed by the cross-validation of the 172\AA\ data sets from Hi-C 2.1. The
ARMCs studied in this paper have characteristic velocities in the range of the
typical sound speeds in coronal loops. Hence, these moving objects differ from
the well-known rapid Alfv\'enic velocity jets from magnetic reconnection sites.
This is also proven by the fact that ARMCs propagate along the active region
magnetic structure (strands). The nature of the discovered statistical grouping
of the ARMC events is not known.
