  Non-potential magnetic energy promptly released in solar flares is converted
to other forms of energy. This may include nonthermal energy of
flare-accelerated particles, thermal energy of heated flaring plasma, and
kinetic energy of eruptions, jets, up/down flows, and stochastic (turbulent)
plasma motions. The processes or parameters governing partitioning of the
released energy between these components is an open question. How these
components are distributed between distinct flaring loops and what controls
these spatial distributions is also unclear. Here, based on multi-wavelength
data and 3D modeling, we quantify the energy partitioning and spatial
distribution in the well observed SOL2014-02-16T064620 solar flare of class
C1.5. Nonthermal emissions of this flare displayed a simple impulsive
single-spike light curves lasting about 20\,s. In contrast, the thermal
emission demonstrated at least three distinct heating episodes, only one of
which was associated with the nonthermal component. The flare was accompanied
by up and down flows and substantial turbulent velocities. The results of our
analysis suggest that (i) the flare occurs in a multi-loop system that included
at least three distinct flux tubes; (ii) the released magnetic energy is
divided unevenly between the thermal and nonthermal components in these loops;
(iii) only one of these three flaring loops contains an energetically important
amount of nonthermal electrons, while two other loops remain thermal; (iv) the
amounts of direct plasma heating and that due to nonthermal electron loss are
comparable; (v) the kinetic energy in the flare footpoints constitute only a
minor fraction compared with the thermal and nonthermal energies.
