  We present 0.95--2.5 micron moderate (R = 500) resolution spectra of 19
ISOCAM detected sources in the Chamaeleon I dark cloud. Thirteen of these stars
are candidate very low mass members of the cloud proposed by Persi et al. (2000
A&A 357:219) on basis of the mid-IR color excess. The sample also includes a
bona-fide young brown dwarf (Cha Halpha 1), a transition
--stellar/sub-stellar-- object (Cha Halpha 2), one previously known T Tauri
star (Sz 33) and three ISOCAM sources with no mid-IR excess. The spectra of the
mid-IR color excess sources are relatively flat and featureless in this
wavelength range. Both atomic and molecular lines (when in absorption) are
partially veiled suggesting the presence of continuum emission from
circumstellar dust. In addition some of the sources show Paschen and Brackett
lines in emission. We apply the 2 micron water vapor index defined by Wilking
et al. (1999 AJ 117:469) to estimate spectral types. These stars have spectral
types M0--8. We use Persi et al.'s stellar luminosity determinations, in
combination with D'Antona & Mazzitelli latest pre-main sequence evolutionary
tracks, to estimate masses and ages. The ISOCAM detected mid-IR excess sources
have sub-solar masses down to the H-burning limit and a median age of few x
10^6 yr, in good agreement with the higher mass members of this cloud.
