  We attempt to model magnetic reconnection during the two-ribbon flare in the
gravitationally stratified solar atmosphere with the Lundquist number of
$S=10^6$ using 2D simulations. We found that the tearing mode instability leads
to the inhomogeneous turbulence inside the reconnecting current sheet (CS) and
invokes the fast phase of reconnection. Fast reconnection brings an extra
dissipation of magnetic field which enhances the reconnection rate in an
apparent way. The energy spectrum in the CS shows the power-law pattern and the
dynamics of plasmoids governs the associated spectral index. We noticed that
the energy dissipation occurs at a scale $l_{ko}$ of 100-200~km, and the
associated CS thickness ranges from 1500 to 2500~km, which follows the Taylor
scale $l_T=l_{ko} S^{1/6}$. The termination shock(TS) appears in the turbulent
region above flare loops, which is an important contributor to heating flare
loops. Substantial magnetic energy is converted into both kinetic and thermal
energies via TS, and the cumulative heating rate is greater than the rate of
the kinetic energy transfer. In addition, the turbulence is somehow amplified
by TS, of which the amplitude is related to the local geometry of the TS.
