  Context. Multi-dimensional solar flare simulations have not yet included
detailed analysis of the lower atmospheric responses such as down-flowing
chromospheric compressions and chromospheric evaporation processes.
  Aims. We present an analysis of multi-dimensional flare simulations,
including analysis of chromospheric up-flows and down-flows that provide
important groundwork for comparing 1D and multi-dimensional models.
  Methods. We follow the evolution of an MHD standard solar flare model
including electron beams, where localized anomalous resistivity initiates
magnetic reconnection. We vary the background magnetic field strength, to
produce simulations that cover a large span of observationally reported solar
flare strengths. Chromospheric energy fluxes, and energy density maps are used
to analyse the transport of energy from the corona to the lower atmosphere, and
the resultant evolution of the flare. Quantities traced along 1D field-lines
allow for detailed comparison with 1D evaporation models.
