WE PROPOSE TO APPROACH THIS GOAL THROUGH THE FOLLOWING PROCESS. WE WILL USE TWO ADVANCED CORONAL MHD MODELS THE RADIATIVE MHD CODE (RADMHD ABBETT W.P. 2007 APJ 665 1469) AND THE MAGNETIC FLUX ERUPTION CODE (MFE FAN 2012 APJ 758 60) AND TOOLS DEVELOPED WITHIN THE CORONAL GLOBAL EVOLUTIONARY MODEL FRAMEWORK (CGEM NASA LWS STRATEGIC CAPABILITY PROJECT FISHER ET AL. 2015 SPW 13 369) TO PERFORM DATA-DRIVEN SIMULATIONS OF TWO FLARING ACTIVE REGIONS. THE ADVANTAGE OF THIS APPROACH IS APPLICATION OF A WELL-TESTED PDFI INVERSION TECHNIQUE TO INFER THE ELECTRIC FIELDS FROM SEQUENCES OF SDO VECTOR MAGNETOGRAMS (KAZACHENKO ET AL. 2014 APJ 795 17) THAT ARE NECESSARY TO DRIVE THE MODELS' PHOTOSPHERIC LAYERS IN A MANNER THAT IS PHYSICALLY CONSISTENT WITH THE OBSERVED EVOLUTION. WE WILL EXPERIMENT WITH DIFFERENT TEMPORAL COMBINATIONS OF CGEM AND MHD RUNS AND WILL ANALYZE HOW DIFFERENTLY SPECIFIED INITIAL AND BOUNDARY CONDITIONS AFFECT THE SIMULATIONS' OUTCOME.