  The Flora family resides in the densely populated inner main belt, bounded in
semimajor axis by the $\nu_6$ secular resonance and the Jupiter 3:1 mean motion
resonance. The presence of several large families that overlap dynamically with
the Floras (e.g., the Vesta, Baptistina, and Nysa-Polana families), and the
removal of a significant fraction of Floras via the nearby $\nu_6$ resonance
complicates the Flora family's distinction in both proper orbital elements and
reflectance properties. Here we use orbital information from the Asteroids
Dynamic Site, color information from the Sloan Digital Sky Survey, and albedo
information from the Wide-field Infrared Survey Explorer to obtain the median
orbital and reflectance properties of the Floras by sampling the core of the
family in multidimensional phase space. We find the median Flora SDSS colors to
be $a^*$ = 0.126 $\pm$ 0.007 and $i-z = -0.037 \pm 0.007$; the median Flora
albedo is $p_V$ = 0.291 $\pm$ 0.012. These properties allow us to define ranges
for the Flora family in orbital and reflectance properties, as required for a
detailed dynamical study. We use the young Karin family, for which we have an
age determined via direct backward integration of members' orbits, to calibrate
the Yarkovsky drift rates for the Flora family without having to estimate the
Floras' material properties. The size-dependent dispersion of the Flora members
in semimajor axis (the "V" plot) then yields an age for the family of
$910^{+160}_{-120}$ My, with the uncertainty dominated by the uncertainty in
the material properties of the family members (e.g., density and surface
thermal properties). We discuss the effects on our age estimate of two
independent processes that both introduce obliquity variations among the family
members on short (My) timescales: 1) the capture of Flora members in spin-orbit
resonance, and 2) YORP-driven obliquity variation.
