  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 \textit{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.
