  The recently observed data by AMS-02 clearly confirms that the positron flux
rises with energy and shows a peak near a few hundred GeV. This rising positron
flux cannot be explained by interactions of cosmic rays with interstellar
hydrogen gas. In this paper, our goal is to study whether secondary production
due to cosmic ray interactions in nearby Galactic Molecular Clouds (GMCs) can
contribute significantly to the observed positron spectrum on Earth. Due to the
progress in multi-wavelength astronomy, many new GMCs have been discovered in
our Galaxy recently. Using large scale CO survey, 1064 GMCs were detected in
the Galaxy, which reside in the Galactic plane. Very recent survey implemented
the optical/IR dust extinction measurements, to trace 567 GMCs within 4 kpc of
Earth, also residing in the Galactic plane. We use the updated list of GMCs
reported in recent papers, which are distributed in the Galactic plane, to find
the secondary positrons produced in them in interactions of cosmic rays with
molecular hydrogen. Moreover, by analysing the \textit{Fermi}-LAT data, new
GMCs have been discovered near the Galactic plane. We also include some of
these GMCs closest to the Earth where cosmic ray interactions are producing
secondaries. It has been speculated earlier that cosmic rays may be
reaccelerated in some GMCs. We select 7 GMCs out of 567 GMCs recently reported,
within 4 kpc of Earth, where reacceleration due to magnetized turbulence is
assumed. We include a hardened component of secondary positrons, produced from
interaction of reaccelerated CRs in those 7 GMCs. We use publicly available
code \textbf{DRAGON} for our simulation setup to study CR propagation in the
Galaxy and show that the observed positron spectrum can be well explained in
the energy range of 1 to 1000 GeV by our self consistent model.
