  We seek to find the precursors of the Herbig Ae/Be stars in the solar
vicinity within 500 pc from the Sun. We do this by creating an optically
selected sample of intermediate mass T-Tauri stars (IMTT stars) here defined as
stars of masses $1.5 M_{\odot}\leq M_* \leq 5 M_{\odot}$ and spectral type
between F and K3, from literature. We use literature optical photometry
(0.4-1.25$\mu$m) and distances determined from Gaia DR2 parallax measurements
together with Kurucz stellar model spectra to place the stars in a HR-diagram.
With Siess evolutionary tracks we identify intermediate mass T-Tauri stars from
literature and derive masses and ages. We use Spitzer spectra to classify the
disks around the stars into Meeus Group I and Group II disks based on their
[F$_{30}$/F$_{13.5}$] spectral index. We also examine the 10$\mu$m silicate
dust grain emission and identify emission from Polycyclic Aromatic Hydrocarbons
(PAH). From this we build a qualitative picture of the disks around the
intermediate mass T-Tauri stars and compare this with available spatially
resolved images at infrared and at sub-millimeter wavelengths to confirm our
classification. We find 49 intermediate mass T-Tauri stars with infrared
excess. The identified disks are similar to the older Herbig Ae/Be stars in
disk geometries and silicate dust grain population. Spatially resolved images
at infra-red and sub-mm wavelengths suggest gaps and spirals are also present
around the younger precursors to the Herbig Ae/Be stars. Comparing the
timescale of stellar evolution towards the main sequence and current models of
protoplanetary disk evolution the similarity between Herbig Ae/Be stars and the
intermediate mass T-Tauri stars points towards an evolution of Group I and
Group II disks that are disconnected, and that they represent two different
evolutionary paths.
