  Solar flares are efficient particle accelerators with a large fraction of
released magnetic energy (10-50%) converted into energetic particles such as
hard X-ray producing electrons. This energy transfer process is not well
constrained, with competing theories regarding the acceleration mechanism(s),
including MHD turbulence. We perform a detailed parameter study examining how
various properties of the acceleration region, including its spatial extent and
the spatial distribution of turbulence, affect the observed electron
properties, such as those routinely determined from X-ray imaging and
spectroscopy. Here, a time-independent Fokker-Planck equation is used to
describe the acceleration and transport of flare electrons through a coronal
plasma of finite temperature. Motivated by recent non-thermal line broadening
observations that suggested extended regions of turbulence in coronal loops, an
extended turbulent acceleration region is incorporated into the model. We
produce outputs for the density weighted electron flux, a quantity directly
related to observed X-rays, modelled in energy and space from the corona to
chromosphere. We find that by combining several spectral and imaging
diagnostics (such as spectral index differences or ratios, energy or
spatial-dependent flux ratios, and electron depths into the chromosphere) the
acceleration properties, including the timescale and velocity dependence, can
be constrained alongside the spatial properties. Our diagnostics provide a
foundation for constraining the properties of acceleration in an individual
flare from X-ray imaging spectroscopy alone, and can be applied to past,
current and future observations including those from RHESSI and Solar Orbiter.
