  To date, we have access to enormous inventories of stellar spectra that allow
the extraction of atmospheric parameters and chemical abundances essential in
stellar studies. However, characterizing such a large amount of data is complex
and requires a good understanding of the studied object to ensure reliable and
homogeneous results. In this study, we present a methodology to measure
homogenously the basic atmospheric parameters and detailed chemical abundances
of over 1600 thin disk main-sequence stars in the 100 pc solar neighborhood,
using APOGEE-2 infrared spectra. We employed the code tonalli to determine the
atmospheric parameters using a prior on log g. The log g prior in tonalli
implies an understanding of the treated population and helps to find physically
coherent answers. Our atmospheric parameters agree within the typical
uncertainties (100 K in Teff, 0.15 dex in log g and $[M/H]$) with previous
estimations of ASPCAP and Gaia DR3. We use our temperatures to determine a new
infrared color-temperature sequence, in good agreement with previous works,
that can be used for any main-sequence star. Additionally, we used the BACCHUS
code to determine the abundances of Mg, Al, Si, Ca, and Fe in our sample. The
five elements (Mg, Al, Si, Ca, Fe) studied have an abundance distribution
centered around slightly sub-solar values, in agreement with previous results
for the solar neighborhood. The over 1600 main-sequence stars atmospheric
parameters and chemical abundances presented here are useful in follow-up
studies of the solar neighborhood or as a training set for data-driven methods.
